Non-Thermal X-ray Emission Properties of Rotation-Powered Pulsars with Chandra & XMM

1. Non-Thermal X-ray Emission Properties of Rotation-Powered Pulsars with Chandra & XMM Xiang-Hua Li Directed by: Ti-Pei Li & Fang-Jun Lu Institute of High Energy Physics, CAS

2. Outline • Introduction & Motivations • Sample and Data process • Results & Discussions • Conclusion

3. Introduction • Rotation powered pulsar radiating at the expense of rotational energy • How the spin-down energy is converted to the high energy radiation? • Many studies have sought to determine the relationship between the X-ray luminosity (Lx) and the spin-down power (Edot)

4. Cheng & Zhang 1999 Radiation Components of Rotation Powered Pulsars • Non-thermal • PWN • pulsed radiation from pulsar • Non-pulsed radiation from pulsar • Thermal • non-pulsed radiation from the pulsar~0.1keV • pulsed radiation from the pulsar~1keV

5. Cheng & Zhang 1999 Radiation Components of Rotation Powered Pulsars • Non-thermal • PWN • pulsed radiation from pulsar • Non-pulsed radiation from pulsar • Thermal • non-pulsed radiation from the pulsar~0.1keV • pulsed radiation from the pulsar~1keV

6. Becker and Trumper (1997) used ROSAT data (0.1-2.4 keV) and found Lx ~ 10-3Edot for 27 rotation-power pulsars (thermal and non-thermal)

7. Saito (1998) used 16 rotation-power pulsars observed by ASCA (2-10 keV) and found Lx ~ (Edot)3/2

8. Possenti et al. (2002) used ROSAT, ASCA, RXTE, BappoSAX, Chandra, XMM (41 pulsars) to obtainLx ~ (Edot)1.34(2-10keV)

9. Motivations • With high spatial resolution X-ray data of Chandra and XMM-Newton data, resolved the pulsar from its surrounding PWNe • Energy range: 2-10keV /exclude thermal components • Check the dependences of Lxand Edot, and other parameters of pulsars and PWNe

10. Sample and data process • All rotation-powered pulsars in the Archived data of Chandra and literatures • Use published spectrum data if available • Process the archived data if unavailable，use XMM data if Chandra sources are too faint • Obtain the X-ray spectrum properties of both pulsar and pulsar wind nebula In Total: 38 pulsars 23 PWNe

11. Results & Discussions

12. Becker&Truemper(1997) ROSAT Possenti et al. (2002) Saito(1998) ASCA The correlation between Lxpsr and Edot of pulsars Lx ~ (Edot)1.34

13. Becker&Truemper(1997) ROSAT Lxpul ~ (Edot)1.15 Cheng (2004) Possenti et al. (2002) The correlation between Lxpsr and Edot of pulsars Lx ~ (Edot)1.34

14. Becker&Truemper(1997) ROSAT Lxpul ~ (Edot)1.15 Cheng (2004) Possenti et al. (2002) The correlation between Lxpsr and Edot of pulsars Theory ：Lx~(Edot)1.15 (Cheng & Zhang 1999) Lx ~ (Edot)1.34

15. Cheng et al. (2004) (Lx)npul ~ (Edot)1.4 Possenti et al. (2002) Saito(1998) ASCA • The correlation between Lx of PWN and Edot Lx ~ (Edot)1.34

16. psr~B psr~c psr~Lx • What these Correlations mean?

17. Conclusions (I) • Lxpsr~Edot relation in 2-10 keV is different from those from 0.1-2.4 keV (Becker & Truemper 1997) • Different emission components • Different energy band • Lxpsr~Edotrelation is different with Possenti(2002) • higher resolution observations have been used • Lxpsr~Edotrelation of pulsars are consistent with the model predicted (Cheng & Zhang 1999)

18. Conclusions (II) • LxPWN~Edot of PWNe are consistent with those given by other authors • The correlations • psr~B • psr~Lxpsr • psr~c What these correlations mean? Welcome suggestions!

19. Thanks